Mass and density of Asteroid 121 Hermione from an analysis of its companion orbit

We report on Adaptive Optics observations of the satellite of Asteroid 121 Hermione with the ESO-Paranal UT4 VLT and the Keck AO telescopes. The binary system, belonging to the Cybele family, was observed during two observing campaigns in January 2003 and January 2004 aiming to confirm its trajectory and accurately determine its orbital elements. A precessing Keplerian model was used to describe the motion of S/2002 (121) 1. We find that the satellite of Hermione revolves at a=768±11 km from the primary in P=2.582±0.002 days with a roughly circular and prograde orbit (e=0.001±0.001, i=3±2° w.r.t. equator primary). These extensive astrometric measurements enable us to determine the mass of Hermione to be 0.54±0.03×¹⁰¹⁹ kg and its pole solution (λ₀=1.5°±2.00, β₀=10°±2.0 in ecliptic J2000). Additional Keck AO observations taken close to the asteroid opposition in December 2003 give us direct insight into the structure of the primary which presents a bilobated shape. Since the angular resolution is limited to the theoretical angular resolution of the telescope (43 mas corresponding to a spatial resolution of 80 km), two shape models (called snowman and peanut) are proposed based on the images which were deconvolved with MISTRAL deconvolution process. Assuming a purely synchronous orbit and knowing the mass of the primary, the peanut shape composed of two separated components is quite unlikely. Additionally the J₂ calculated from the analysis of the secondary orbit is not in agreement with the peanut model, but close to the snowman shape. The bulk density of the primary as derived from the observed size of the snowman shape is estimated to ρ∼1.8±0.2 g/cm³ implying a porosity ∼14% for this C-type asteroid, corresponding to a fractured asteroid. Considering the IRAS diameter, the density is lower (ρ=1.1±0.3 g/cm³) leading to a high porosity (p=30-60%) with a nominal value of p=48%, which indicates a completely loose rubble-pile structure for the primary. Further work is necessary to better constrain the size, shape, and then internal structure of Hermione's primary.     

M31的观测与研究进展

介绍了本星系群中最大的旋涡星系M31(仙女星系)的基本观测性质。与银河系结构类似，M31的基本成分包括：核、核球、盘和晕。对以上各个成分的观测和研究进展分别作了综述，重点是盘的星族成分和恒星形成历史，以及球状星团的分布和晕的形成历史。同时与银河系的各种观测特征和形成机制作了详细的比较。     

HAXTEL: A Laue lens telescope development project for a deep exploration of the hard X-ray sky (> 60 keV)

A review of the HAXTEL project devoted to the development of a Laue lens telescope for hard X-/gamma-ray observation of the continuum spectra of celestial sources is presented. Main design properties, open issues, the status of the project and an example of multi-lens configuration with sensitivity expectations are discussed.     

利用GPS组合观测值探测修复周跳的方法比较

在目前常用的周跳探测与修复方法基础上,分析利用GPS组合观测值来探测修复周跳的3种方法,通过模拟的实验结果证明其有效性,比较各个方案的特性,并引入LC-PC衡量标准比较各方案探测修复周跳的能力。     

分布式水文模型的GPU并行化及快速模拟技术

分布式水文模型对流域水文过程的应用深度及广度不断加深,常与数值天气及气候预报相结合,面临巨大的计算量。近年来GPU技术的进步使普通电脑能够实现高效而又廉价的并行计算。提出了资料插值、单元产流以及单元汇流采用GPU并行计算,马斯京根法河道汇流采用一种非并行的递归方法。基于笔记本电脑和NVIDIA GPU/CUDA结合C#语言,由分布式新安江模型在沂河流域的模拟应用表明,降水量空间插值及新安江产流的并行执行效率为普通CPU上C#的8~9倍。使用直接递归法实现马斯京根汇流演算比以往采用汇流次序表的执行效率提升0.5~0.9倍。     

网络并行电法与传统电法超前探测效果对比

网络并行电法是以分布式并行智能电极电位差信号采集方法为技术核心支撑的直流电法,其数据采集模拟地震勘探方式进行,与常规电法每次供电只能采得一个测点数据不同,并行电法每次供电可同时获得多个测点数据,是一种全电场观测技术。运用两种方法对龙岩市新罗区大弯煤矿和武平荧石矿进行超前探测试验对比研究,并经实际巷道掘进揭露验证,表明网络并行电法技术较传统电法技术效果更好,效率更高。     

一种基于横向或纵向扫描线处理的填洼算法

针对传统PlanchouDarbous算法采用递归执行方式导致处理效率低下等问题,该文提出了一种适合基于CUDA的GPU并行执行的DEM洼地填充算法。此算法采用淹没-排水思路,多次推进式扫描完成排水;在串行执行和并行执行两种方式下,算法处理有所差异,其中串行算法代码更短;串行算法的时间复杂度为O(n),测试结果表明串行执行时快于PlanchonDarboux算法,且在CUDA环境下的并行执行用时不到串行执行用时的一半。算法思路简单,易于编程实现。